SWG 19: Pasadena PLASTIC Status Report Toni Galvin M. Popecki, - - PowerPoint PPT Presentation
SWG 19: Pasadena PLASTIC Status Report Toni Galvin M. Popecki, K. Simunac, B. Klecker L. Kistler, L. Ellis, C. Farrugia, E. Moebius, Y. Liu M. Lee, J. Barry, P. Bochsler, P. Wurz, L. Blush 1 R. Wimmer-Schweingruber, A. Opitz, L. Berger
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due to delivery timing of some memory register commands
Two previously unknown problems; both needed to create the hangup:
– Leap-year error in the POC s/w (since corrected by UCB, thanks!) + – Variation in S/C from MOC-POC ICD about handling time-tag commands
3/3/08 - DPU FSW load 3.2.7 11/19/08 MCP HV increase - 20V 11/21/08 Raised DPU-side S-ch switch threshold 11/26/08 MCP HV increase - 20V
Temporal Evolution of the Solar Wind during the Recent Solar Minimum: Observations and Consequences for Space Weather Modeling Applications of Grad-Shafranov Reconstruction Techniques on Magnetic Clouds Observed by Stereo and Wind and Comparison to Solar Source Interstellar Pickup Ion Observations by STEREO: Focus Cone Variations with Solar Wind Streams High Resolution Minor Ion Composition and Kinetic Properties at Solar Wind Interfaces -- Solar Source Back Mapping Suprathermal Ions in Compression Regions and in Upstream Events
Reference: (1) M. Leitner, C. J. Farrugia, A. B. Galvin, H. K. Biernat, and V.
STEREO A and B at solar minimum 2007, and comparison with two other minima, Solar Phys., under review, 2009.
Is the Current Solar Cycle Minimum Weaker than Previous Cycles? STEREO - Wind - Heiios Observations of the Solar Wind QI The solar wind quasi-invarient (QI) is the ratio of the solar magnetic wind magnetic energy density to the plasma kinetic energy density, that is, the inverse square of the Alfven Mach number. QI complements other indices and has implications on the Sun-Solar System connection during an entire solar activity phase. On average, the QI(2007) is less than that
indicating weaker solar activity. This also implies weaker MHD effects in solar wind flow around planetary magnetospheres which, in turn, alters the flow’s interaction with them.
References: (1) A. Opitz et al., Temporal evolution of the solar wind bulk velocity at solar minimum by cross-correlating the STEREO A and B PLASTIC measurements, Solar Phys., accepted, 2009. (2) J.J. Podesta, A.B. Galvin, C.F. Farrugia, Correlation length of solar wind fluctuations measured tangent to the earth’s orbit: First results from STEREO, J. Geophys. Res., 113, A09 104, doi: 10.1029/2007JA012865, 2008. (3) K.D.C. Simunac, et al., In Situ Observations of Solar Wind Stream Interface Evolution, Solar Phys., under review, 2009.
Temporal Evolution of the Solar Wind during the Recent Solar Minimum: Observations and Consequences for Space Weather Modeling The heliocentric orbits of the two STEREO satellites provide a unique opportunity to study the cross-correlation of solar wind parameters1,2, and, during these solar minimum conditions, the evolution of stream interfaces3 near 1 AU over time scales of hours to a few days, that is, much less than the period of a Carrington rotation. Presentation this SWG by Kristin Simuanc
Applications of Grad-Shafranov Reconstruction Techniques
and Wind Comparison to Solar Source Multi-spacecraft STEREO and Wind
clouds (MCs) with increased accuracy. The model was a Grad-Shafranov Reconstruction where data from two spacecraft were ingested to
spacecraft where about 9o apart. For one MC it was possible to compare the magnetic flux content with that inferred from the corresponding two-ribbon flare on the Sun. For the first time it was shown that most of the magnetic flux of the MC, now better constrained because of the available multi- spacecraft observations, is created during the eruption on the Sun.
References: (1) Kilpua, E., P. Liewer, C. J. Farrugia, J. G. Luhmann, C. Moestl, et al., Multi-spacecraft observations of magnetic clouds and their solar origins: May 19ｭ23, 2007, Solar Phys., in press, 2009. (2) C. Moestl, C. J. Farrugia, C. Miklenic, M. Temmer, A. B. Galvin, J. G. Luhmann, et al., Multi-spacecraft recovery of a magnetic cloud and its
2009. (3) C. Moestl, C. J. Farrrugia, M. Leitner, E. K. J. Kilpua, A. B. Galvin, et al., Optimized reconstruction of a small magnetic cloud using STEREO-WIND
The shape of the magnetic clouds in a plane perpendicular to the invariant axis is composed of field lines showing a deformed elliptical shape (yellow sphere is the Sun, the spacecraft are from left to right: STEREO- B, WIND (Earth), STEREO-A) .
Interstellar Pickup Ion Observations by STEREO: Focus Cone Variations with Solar Wind Streams Pickup helium ions provides diagnostics for Local Interstellar Cloud parameters, such as the LIC flow velocity vector and temperature. However, pickup ion distributions are highly variable and are known to be affected by the interplanetary magnetic field, solar wind density, ionization rates & probably several unknown causes. For deduction of LIC parameters, mitigation is sought with better information to distinguish temporal vs spatial
STEREO RESULTS: Presentation this SWG by Berndt Klecker
References: (1) B. Klecker et al., AGU 2008, SWG 2009 (2) E. Moebius, B. Klecker et al. Simultaneous Pickup Ion Observations of the Interstellar Helium Focusing Cone with STEREO PLASTIC A & B, Cospar 2008.
Cut-off
Data available through SSC web-site:
All Level 1 CDF: Housekeeping, monitor rates, and all science data, including proton
ion efficiencies. (These files are used in analysis programs SPLAT and PHA_PLAY.) Level 2 CDF 1-minute cadence data for the 1D- Maxwellian derived proton bulk
because they require the *.fin Level 0 files. Data: epoch, epoch_1kev, error codes, caution codes, s/c attitude flag, proton density, proton bulk speed, kinetic temperature, thermal velocity, n_s_flow_angle, carrington_rotation, spcrft_lon_carr, heliospheric_dist, spcrft_lon_hee, spcrft_lat_hee, spcrft_lon_heeq, spcrft_lat_heeq, spcrft_lon_hci, spcrft_lat_hci. New STA processing this week, to incorporate E_W flow angle, and velocity components (RTN, HERTN).
Data Plots
Ascii/Excel Proton bulk parameters: 1 min (4/2007-9/2008), 10 min (2/2007-9/2008), 1 hr (2007-7/2008) Automatically Generated Plots: Level 2 Proton Moments (1D Max) Bulk Vel, Density, Temperature, and Thermal_vel through present On-Board Moments: Bulk Vel, Density, Temperature, Vel. Standard Deviation through present Solar Wind Stack Plots through 10/2008 He+ Survey Plots through present Spacecraft roll, pitch, and yaw through present Movie: Solar Wind Fe Charge States at CIR Coming this week: STA Proton Velocity Components
STEREO Team meeting April 7-9 2009, to be held in Concord NH at the STEREO EPO Partner McAuliffe-Sheppard Discovery Center
please contact
berndt.klecker@mpe.mpg .de